. Epoch of reionization . Recombination . Peak star formation Inflation Astroparticle era . Recombination . Epoch of reionization . Peak star formation

Take this to the next stage 4 claims in the NoI first SNe first SMBH detect LSS change due to reionization serendipitous transients Take this to the next stage Astrophysics Simulation Experiment design Results and Analysis

ERS NoI Just as a well publicized early goal of HST was to measure the Hubble Constant, so a well publicized early goal of JWST is to find and characterize the first stars in the Universe. But Population III does not come with a handbook of how to do this. JWST takes us into a discovery space of transient phenomena at AB∼27 mag of which we have no knowledge. The community needs to know what is there, as it may affect the subsequent mission in significant ways. SNe are the defining characteristic of Pop III. When the first SNe occur, Pop III ends, because the first metals have been injected into the IGM. Inter alia the First Transients ERS may recognize the first supernovae by their rise time. If this was achieved, it would open up a wealth of follow up science for the community , not fully predictable at the time of launch, but possibly among the major outcomes of the mission.

Astrophysics plan for May What are the core collapse rates ? including SLSN What are the SNIa rates ? Jos. Vinko What are the DCBH rates ? Dan Whalen

Simulation plan for May DRAGONS Paul STIPS Avishay and Armin Rest ADDSTAR Jeremy DRAGONS needs SN rates including Can Anton get us a pre-release version of STIPS?

Experimental design Lifan Will GOODS N allow us to obtain 400 sq arcmin two epochs during the ERS period ? Are there better field choices ? Optimize exposure time with APT including NIRSS parallel exposures Shall we invest 10% of our time in NIRSpec ?

Results and Analysis How many SNIa can we detect and what do they look like ? SLSNe z (6,10) are transients with z dropout hosts Do we expect to see any ? SNe z (10,30) are K dropout transients Can we see any in 5 years of JWST? AGN = blue transients. Link DCBH rate with these

White paper issues DCBH white paper section can be written by Lifan and Dan and Anton Trade off between area and depth. Anton & Lifan Include brown dwarf foreground Jeremy Galaxies Can we detect change in PS between z=10 and z=6? WF survey good for finding the first red galaxies

White paper section on DCBH Born starving Whalen Alvarez 2006 kicks, gas loss Ly a emitter at z 7 CR7 monolithic collapse of halo Woods 2017, Hammerle 2017 in prep GR collapse during H burning Cold flows Di Matteo 2011 ApJ Metallicity comes out solar Next step: synthetic observables AB H 18 for z=7 Rates Djikstra and Yue et al (GRB rates)

Whitepaper notes on SNe SNIa section by J. Vinko Ia rate drops to zero at z =2 w/o prompt Peter & Joszef should write up SLSN at high z SLSN need longer than the ERS to find Hard to map SLSN into a specific mass  range Peter Nugent said whatever mag gain you get from lensing is lost in drop in volume AGN are blue according to Volker Bromm Hummel 2012 ApJ 755 PISN rates (more references)

Other issues to pursue Kasen has very high SN rates Figure of merit: million Mpc3 there are 20 Mpc3 per sq deg between z 6,7 Very high DCBH rates in Habouzit et al Probably don’t need Ariel Goobar or Peter Nugent to do the cluster lensing simulation

Subaru proposal Jeremy SSP UltraDeep (equatorial = unsuitable) SXDS (02 : 18 : 15.60,−04 : 51 : 00.00) Cosmos. (10 : 00 : 28.60,+02 : 12 : 21.00) ElaisN1 is a +50 Deep field Need a Japanese PI Kilonovae are merging NS, ejecta >0.1c, Masaomi Tanaka 1000 per Gpc3 per yr The minimum # women you can have on an ERS team is 10%

Other tasks suggested by A & J WP0 set up a web page WP1 including background WP2 James Webb Transient Factory design ERS learning experience for JWTF Project Manager

Science and deliverables The ERS mantra is to enable the community to play with JWST data ASP after launch A better approach: JWST performance is incorporated into TAO Proposers test their observing plans with TAO Does the planned data test the observer’s hypothesis?

The Theoretical Astrophysical Observatory (TAO) Simulation database Web form data query Image generation Telescope simulator Light cone generation SEDs + Filters Bringing cosmological simulations and galaxy formation models to every astronomer Opened March 2014 Registered users: 300+ Virtual universes built: 400+

TAO https://tao.asvo.org.au Telescope simulator Image generation Simulation database Web form data query Image generation Telescope simulator Light cone generation SEDs + Filters https://tao.asvo.org.au

> Cosmological dark matter simulations > Galaxy formation & evolution models > Mock survey light cones > Mock images of galaxies > Understand and interpret the observations

through NeCTAR, NCRIS and EIF funding. The TAO project is part of the ASVO NeCTAR Virtual Laboratory, supported by Swinburne University, Astronomy Australia Limited, and the Commonwealth Government through NeCTAR, NCRIS and EIF funding. http://tao.asvo.org.au http://www.asvo.org.au https://www.nectar.org.au/all-sky-virtual-observatory

Low redshift predictions for the distribution of cosmic gas z=0 z=0.1 z=0.2 z=0.3 Low redshift predictions for the distribution of cosmic gas z=1

High redshift predictions for the spectra of distant galaxies z=1 z=2 z=3 z=0 z=1

TAO light-cone module

The TAO image module

Videogame view of ERS Scientific view of ERS To allow the community to play with JWST data from as soon as possible after launch Scientific view of ERS To allow the community to conceptualize new experiments with JWST as soon as possible after launch This is most effective if the concepts are immediately trialed on the Theoretical Astrophysical Observatory

Donald Trump was right….. The Hubble Deep Field was the great achievement of HST